Abstract
Ionization of the atmosphere of Titan by galactic cosmic rays is a very significant process throughout the altitude range of 100 to 400 km. An approximate form of the Boltzmann equation for cosmic ray transport has been used to obtain local ionization rates. Models of both ion and neutral chemistry have been employed to compute electron and ion density profiles for three different values of the H 2/CH 4 abundance ratio. The peak electron density is of the order 10 3 cm −3. The most abundant positive ions are C 2H 9 + and C 3H 9 +, while the predicted densities of the negative ions H − and CH 3 − are very small (<10 −4 that of the positive ions). It is suggested that inclusion of the ion chemistry is important in the computation of the H and CH 3 density profiles in the lower ionosphere.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
